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Dynamical Evolution of Viscous Disks around Be Stars. I: photometry
Solar and Stellar Astrophysics · Submitted 11 Jul 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that lightcurves for different wavelengths are specific of a mass loss history, inclination angle and $\alpha$ viscosity parameter.
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The abstract, sentence by sentence
Be stars possess gaseous circumstellar disks that modify in many ways the spectrum of the central B star. Furthermore, they exhibit variability at several timescales and for a large number of observables. Putting the pieces together of this dynamical behavior is not an easy task and requires a detailed understanding of the physical processes that control the temporal evolution of the observables. There is an increasing body of evidence that suggests that Be disks are well described by standard $\alpha$-disk theory. This paper is the first of a series that aims at studying the possibility of inferring several disk and stellar parameters through the follow-up of various observables. Here we study the temporal evolution of the disk density for different dynamical scenarios, including the disk build-up as a result of a long and steady mass injection from the star, the disk dissipation that occurs after mass injection is turned off, as well as scenarios in which active periods are followed by periods of quiescence. For those scenarios, we investigate the temporal evolution of continuum photometric observables using a 3-D non-LTE radiative transfer code. We show that lightcurves for different wavelengths are specific of a mass loss history, inclination angle and $\alpha$ viscosity parameter. The diagnostic potential of those lightcurves is also discussed.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Be stars possess gaseous circumstellar disks that modify in many ways the spectrum of the central B star. | background 1.00 | 0.06 | 0.02 | asserted 1.00 |
| s1 | Furthermore, they exhibit variability at several timescales and for a large number of observables. | background 1.00 | 0.08 | 0.02 | asserted 1.00 |
| s2 | Putting the pieces together of this dynamical behavior is not an easy task and requires a detailed understanding of the physical processes that control the temporal evolution of the observables. | background 0.75 | 0.05 | 0.02 | asserted 0.99 |
| s3 | There is an increasing body of evidence that suggests that Be disks are well described by standard $\alpha$-disk theory. | background 1.00 | 0.05 | 0.04 | hedged possibility 1.00 |
| s4 | This paper is the first of a series that aims at studying the possibility of inferring several disk and stellar parameters through the follow-up of various observables. | contribution 0.58 | 0.34 | 0.04 | asserted 0.60 |
| s5 | Here we study the temporal evolution of the disk density for different dynamical scenarios, including the disk build-up as a result of a long and steady mass injection from the star, the disk dissipation that occurs after mass injection is turned off, as well as scenarios in which active periods are followed by periods of quiescence. | contribution 0.90 | 0.79 | 0.04 | asserted 0.91 |
| s6 | For those scenarios, we investigate the temporal evolution of continuum photometric observables using a 3-D non-LTE radiative transfer code. | method 0.98 | 0.91 | 0.03 | asserted 0.96 |
| s7 | We show that lightcurves for different wavelengths are specific of a mass loss history, inclination angle and $\alpha$ viscosity parameter. | result 1.00 | 0.93 | 0.71 | asserted 1.00 |
| s8 | The diagnostic potential of those lightcurves is also discussed. | interpretation 0.86 | 0.56 | 0.08 | unclear 0.82 |
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Original abstract
Be stars possess gaseous circumstellar disks that modify in many ways the spectrum of the central B star. Furthermore, they exhibit variability at several timescales and for a large number of observables. Putting the pieces together of this dynamical behavior is not an easy task and requires a detailed understanding of the physical processes that control the temporal evolution of the observables. There is an increasing body of evidence that suggests that Be disks are well described by standard $\alpha$-disk theory. This paper is the first of a series that aims at studying the possibility of inferring several disk and stellar parameters through the follow-up of various observables. Here we study the temporal evolution of the disk density for different dynamical scenarios, including the disk build-up as a result of a long and steady mass injection from the star, the disk dissipation that occurs after mass injection is turned off, as well as scenarios in which active periods are followed by periods of quiescence. For those scenarios, we investigate the temporal evolution of continuum photometric observables using a 3-D non-LTE radiative transfer code. We show that lightcurves for different wavelengths are specific of a mass loss history, inclination angle and $\alpha$ viscosity parameter. The diagnostic potential of those lightcurves is also discussed.
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References
How the literature uses it
2 arXiv papers cite this in 2 sentences
What it cites
Cites as support 2 papers
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Spectrointerferometry and spectroastrometry are starting to provide clear evidence that, in most observed and so far analyzed systems [ref] , the disks rotate in a Keplerian fashion [ref] .
Gas Distribution, Kinematics, and Excitation Structure in the Disks around the Classical Be Stars Beta Canis Minoris and Zeta Tauri · Introduction · 0.96
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Spectrointerferometry and spectroastrometry are starting to provide clear evidence that, in most observed and so far analyzed systems [ref] , the disks rotate in a Keplerian fashion [ref] .
First spectro-interferometric survey of Be stars I. Observations and constraints on the disks geometry and kinematics · Introduction · 0.96
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